Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9-662446 in the Large Magellanic Cloud

TL;DR

This study reports the discovery of a new Be/X-ray binary pulsar in the Large Magellanic Cloud, characterized by a 1412-second spin period and an orbital period of about 151 days, using multi-wavelength observations.

Contribution

The paper presents the first identification and detailed analysis of a Be/X-ray binary pulsar in the LMC, including timing, spectral, and optical observations, expanding knowledge of HMXB populations.

Findings

Detected a pulsar with a 1412 s spin period.

Estimated an orbital period of approximately 151 days.

Confirmed the source as a Be X-ray binary in the LMC.

Abstract

Context. The Magellanic Clouds are our nearest star-forming galaxies. While the population of high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) is relatively well studied, our knowledge about the Large Magellanic Cloud (LMC) is far from complete given its large angular extent and insufficient coverage with X-ray observations. Aims. We conducted a search for new HMXBs in the LMC using data from eROSITA, the soft X-ray instrument on board the Spektrum-Roentgen-Gamma (SRG) satellite. Methods. After confirming the nature of eRASSU J052914.9-662446 as a hard X-ray source positionally coincident with an early type star, we followed it up with optical spectroscopic observations from South African Large Telescope (SALT) and a dedicated NuSTAR observation. Results. We study the broadband timing and spectral behaviour of the newly discovered HMXB eRASSU J052914.9-662446 through eROSITA, Swift and NuSTAR data in X-rays and the Optical Gravitational Lensing Experiment (OGLE) and SALT RSS data at optical wavelength. We report on detection of the spin period at 1412 s and suggest an orbital period of the system of ~151 days, and thereby establish eRASSU J052914.9-662446 as an accreting pulsar. Further, through optical spectroscopic observations and the existence of H alpha emission the source is identified as a Be X-ray binary pulsar in the LMC. We also investigate the variability of the source in the optical and X-ray regime over the last decades and provide estimates on the possible magnetic field strength of the neutron star.